2019-07-31T08:47:34.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE SOT Demoto Okamoto DeRosa (RCO) -> Okamoto 81 Synoptic Sun Center DC, SYN DC, SYN 19 18 25 327 163 2015-03-06T17:57:31.000Z 2015-03-06T17:57:55.000Z 18 25 Synoptic Synoptic BFI NFI (revised: small, no mask, Na D cont.) The objectives of these observations are to observe the evolution of the magnetic field distribution around the poles during the solar cycle, and to understand the relationship between photospheric magnetic field and the coronal structures (include the solar wind) around the poles. The polar observations by SOT/SP revealed that there are many strong patchy magnetic poles around the poles. Such strong magnetic fields in the polar region may strongly relate with the dynamo and it is very important to observe the evolution of the magnetic field distribution for understanding the dynamo. The strong patchy magnetic poles have the trumpet-like vertical magnetic structure. Although we think that the trumpet structures may relate with the fast solar wind, there are no coronal (X-ray/EUV) structures on most of the magnetic structures. To understand the fast solar wind, the relationship between photospheric magnetic fields and coronal structures in the polar coronal hole is very essential. During the polarity reversal, the opposite polarity magnetic field invade the polar region. At the time, the relationship between coronal activities/structures and photospheric magnetic field is very interesting for understanding the solar wind. ivo://sot.lmsal.com/VOEvent#2015-03-06T17:57:00Z